HIP 41378 Archives

Artist’s rendering of the system around the star HIP 41378. The rings around HIP 41378 f have not been confirmed. Crédit : Salomé Grouffal

A System Of At Least Six Exoplanets Revealed In The HIP 41378 System

by Keith CowingJuly 15, 2026July 15, 2026

[Paris Observatory] An international team, including scientists from the Paris Observatory – PSL at the Time-Space Laboratory, has spent ten years studying an exceptional planetary system comprising at least six […]

Light curves of HIP 41378. Upper panel: K2 C5 campaign (long cadence). Bottom panel: K2 C18 campaign (short cadence). The pink curve represents the median of the best-fit model from photometry and RV analysis. The names of the planets are highlighted with their letters. -- astro-ph.EP

A Decade Of Monitoring The HIP 41378’s Planetary System

by Keith CowingJune 25, 2026June 25, 2026

Multi-planetary systems provide key constraints on planet formation and evolution, as their architecture encodes the dynamical history of planets formed within a common protoplanetary disk.

Long- and short-cadence transit light curve data for HIP 41378 f, folded with orbital period Porb = 542.08 days. The reduced long-cadence data is shown in the left panels in scattered points; the short-cadence data is shown on the right with small points, then binned to 30 minutes and plotted with large points. The solid purple curve shows a randomly-drawn model from the posterior for comparison. The lower row presents the residual between the maximum likelihood model and the data. If we select the maximum likelihood model with f > 0.1, we obtain the residual shown in the dashed purple curve, which is disfavored with log-likelihood difference ∆ (log L) ≈ −3.4 -- astro-ph.EP

Astronomy & Telescopes, Exoplanets, -moons, -comets, Imaging & Spectroscopy, Status Report

A Long Spin Period For A Sub-Neptune-mass Exoplanet

by Keith CowingFebruary 23, 2025February 23, 2025

HIP 41378 f is a sub-Neptune exoplanet with an anomalously low density. Its long orbital period and deep transit make it an ideal candidate for detecting oblateness photometrically.